Once CO is released, we find that its dynamics is different from that modelled in extrasolar systems so far (see Appendix ), i.e., the gas does not evolve viscously inwards as expected in massive disks [1]}. It is due to two reasons. First the gas quantity we find in the KB is very small and not in the fluid regime in contrast to systems detected up to now. Second, the majority of gas detections has been around A-type stars [2]}, where stellar winds are not important (only stars cooler than about F5 possess significant convective envelopes and then magnetic fields that can produce strong stellar winds). In contrast, in the Solar System, the Solar wind (SW) drives the dynamics of the gas. We find that once released, CO gets pushed outwards by SW protons on timescales of a few years (at a rate between \(\sim 3\)  to 10 au/yr depending on the location, see Appendix ). Some of this CO gets dissociated and ionized (when interacting with SW protons, photons from the Sun and/or the interstellar medium, see Appendix ) on its way out. However, the ionization and dissociation timescales are of order 100 yr so that CO remains the dominant species up to \(\sim 500\)  au (see Appendix ), i.e. well beyond the heliopause (which is the boundary of the heliosphere where the Solar wind is stopped by the interaction with the local interstellar medium) at \(\sim \)  150 au [3]}. The daughter products of the CO dissociation, namely C and O, are ionized in \(\sim \)  100 yr, leading to an ionized atomic component beyond \(\sim \)  500 au. These ions will then follow the interstellar magnetic lines and get ejected further in the interstellar medium (see Appendix ). The model predictions for CO, C, O (neutral and ionized) as a function of distance to the Sun are shown in Fig. REF  and a summary of the model is given in Appendix .
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